With the latest advancements in our knowledge of spectral modelling, multi-temperature biases, and/or instrumental calibration, current measurements thus favour a uniform chemical composition over the entire volume of clusters and groups, as early suggested for the cores of both systems (and ellipticals) by [1]}. Interestingly, in both regimes the chemical composition is also remarkably close to that of our own Solar System. Indeed, Hitomi confirmed that all the investigated X/Fe ratios of the Perseus Cluster are consistent with Solar at very high precision [2]}, [3]}, and detailed investigations of the CHEERS sample found the same trend for groups and ellipticals as well [4]}, [5]}. This is further illustrated in Fig. REF , where we compiled the average chemical composition of the 21 CHEERS low-mass systems.
